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Computational Astrophysics

In simulations of a star-disk system in the closest vicinity of a star, we
obtain very fast, light ejecta of matter. Those micro-ejections are of small
mass and angular momentum flux, and can be launched from a resistive
magnetosphere above the disk gap. Shown is the absolute value of toroidal
current in code units, in logarithmic color grading. In solid lines are
drawn poloidal magnetic field lines, with lines along which magnetic field
vector points towards the star painted in black color, and those where the
field points in the opposite direction, in white color. Reconnection is
ongoing along the boundary sheet between the opposite-directed magnetic
fields. The quasi-stationary state is reached, with matter pushed out of the
magnetosphere by pressure gradient and magnetic forces, helped by
reconnection. Vectors show poloidal velocity, normalized to Keplerian
velocity at R=2.8 (for more details, see Cemeljic et al., 2013, ApJ768, 5).